Chapter 6: Our Solar System and Its Origin

Transcription

1 Chapter 6: Our Solar System and Its Origin

2 What does our solar system look like?

3 The planets are tiny compared to the distances between them (a million times smaller than shown here), but they exhibit clear patterns of composition and motion. The patterns are far more important and interesting than numbers, names, and other trivia!!

4 The scale of the solar system On a 1-to-10 billion scale: Sun is the size of a large grapefruit (14 cm). Earth is the size of a ball point, 15 meters away. The average distance from the Earth to the Sun defined to be one Astronomical Unit (about 150 million kilometers). Pluto (the most distant planet in our solar system) is about 600 meters away (1/3 of a mile).

6 Mercury (0.4 AU from the Sun) made of metal and rock; large iron core no atmosphere very hot and very cold: 425 C (day), 170 C (night)

7 Venus (0.7 AU) nearly identical in size to Earth extreme greenhouse effect even hotter than Mercury: 470 C, both day and night atmospheric pressure equiv. to 1 km deep in oceans no oxygen, no water, how did it end up so different from Earth?

8 Earth and Moon to scale Earth (1 AU) An oasis of life The only surface liquid water in the solar system about 3/4 of surface covered by water A surprisingly large moon

9 Mars (1.5 AU) Looks Earth-like, but Cold rocky planet with little atmosphere Water flowed in the distant past: could there have been life?

11 The moons are miniature planets and as interesting as Jupiter itself The four Galilean moons Io has active volcanos Europa icy surface + subsurface ocean? Ganymede largest moon in the S.S. Callisto large ice ball w/craters

17 Uranus (19.2 AU) much smaller than Jupiter/Saturn, but still much larger than Earth made of H/He gas and hydrogen compounds (H 2 O, NH 3, CH 4 ) extreme axis tilt: nearly tipped on its side

18 Neptune (30.1 AU) Very similar to Uranus (but much smaller axis tilt) Many moons, including unusual Triton: orbits backward

19 Pluto (39.5 AU) A misfit among the planets: far from Sun like large jovian planets, but much smaller than any inner, terrestrial planet. Comet-like composition (ices, rock) and orbit (eccentric, inclined, 248 years period). Large Moon (Charon)

20 Planetary data table

21 Planetary data table

22 Planetary data table

23 Planetary data table

24 Planetary data table

25 Planetary data table

26 What are the clues to our solar system s formation? Patterns of motion (organized) Composition (differentiated between terrestrial and Jovian) Asteroids and comets (remnants of the formation process) Anomalies (massive, random impacts in early solar system)

27 1. The Sun, all planets, and all large moons orbit and rotate in an organized way. Counterclockwise, as seen from above the north pole (right hand rule)

28 2. Terrestrial planets are small, rocky, and close to the Sun. Jovian planets are large, gas-rich, and far from the Sun. (What about Pluto?)

37 4. A successful theory of solar system formation must explain the major trends, but also allow for exceptions to rules.

38 Summary: Four Major Features of our Solar System

39 How did the solar system form?

40 According to the nebular theory, our solar system formed from the gravitational collapse of a giant cloud of interstellar gas. (nebula = cloud in Latin)

41 The cloud of gas that gave birth to our solar system resulted from the recycling of gas through many generations of stars within our galaxy.

42 Stars are born in molecular clouds Clouds are very cold: ~10-30 K. (273 K = water freezes) Stars form when gravity overcomes thermal pressure. Then gas clumps begin to collapse.

43 Earliest stages of star birth Dense cores of gas in the larger molecular cloud collapse due to self-gravity. Cloud heats up as it contracts due to conservation of energy: gravitational potential energy is converted to thermal energy (heat).

44 Rotation is an important factor during the star birth process (part 1) As gravity forces a dense core to become smaller, it spins faster and faster. This is due to conservation of angular momentum. Dense cores have a small amount of initial rotation. As the cores get smaller, they must spin up to conserve angular momentum.

45 Rotation is an important factor during the star birth process (part 2) Collisions between gas particles in cloud gradually reduce random motions and up+down motions. Collisions flatten the cloud into a disk. The result is a rotating protostar with a rotating disk of gas & dust. The orderly motions of our solar system today are a direct result of the solar system s birth in a spinning, flattened cloud of gas.

46 As gravity causes cloud to shrink, its spin increases (conservation of angular momentum). Spinning cloud also flattens as it shrinks.

47 Collisions between gas particles in cloud gradually reduce random motions. Initial gas cloud has motions of all different ellipticities. But at the end, only circular orbits remain.

48 Spinning cloud flattens as it shrinks.

49 Orderly motions of our solar system today are a direct result of the solar system s birth in a spinning, flattened cloud of gas.

50 Disks around other stars: Solar systems in the making Nearby star-forming regions have 1000 s of young (few Myr) stars. Most of them (~2/3) have disks of gas & dust around them, which are the birthplaces for other solar systems.

51 Disks around other stars: Solar systems in the making Plenty of evidence for spinning disks of gas and dust around other stars, especially around newly formed (few Myr) stars.

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